1. A Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy’s Evolution (SAGE) Bob Blum and the SAGE Team http://sage.stsci.edu/ Image credit, Karl Gordon

2. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 2 The SAGE team ( http://sage.stsci.edu/) Space Telescope Science Institute: Meixner (PI, database lead), Leitherer (team web page), Nota, Panagia, Vijh University of Wisconsin: Churchwell (IRAC pipeline lead), Meade, Babler, Bracker, Gallagher SSI: Whitney (star formation co-lead) University of Arizona: Gordon (MIPS pipeline lead), Engelbracht, Misselt, For, Zaritsky, Harris, Kelly, Perez Spitzer Science Center/JPL: Reach (ISM co-lead), Latter, van Dyk, Werner, Gorjian NOAO: Blum (Evolved star lead), Olsen, Mould, Points Nagoya University, Japan: Onishi, Fukui, Kawamura, Mizuno, Mizuno (CO survey), Shibai (ASTRO-F), Shuji (Near-IR survey) CESR/Saclay/IAS: Bernard (ISM co- lead), Madden, Boulanger, Paladini UC Berkeley: Cohen (calibration) University of Virginia: Indebetouw (star formation co-lead) Harvard/CfA: Hora NASA/Ames: Tielens (IRS) Gemini: Volk University of Michigan: Oey University College London: Smith AURA: Frogel CSIRO: Staveley-Smith JHU: Srinivasan University of Denver: Ueta Manchester: Markwick-Kemper (IRS)

3. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 3 The Large Magellanic Cloud Galaxy Formation & Evolution – 50 kpc – 10 10 Msun – 10 8 Msun in gas – SFR ~ 0.5-1 Msun/yr

4. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 4 Detailed SFHs Smecker-Hane et al., 2002

5. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 5 Detailed SFH's Smecker-Hane et al., 2002 SFR (Msun/yr/sqdeg) Age (Gyr)

6. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 6 Putman, M. (2000) Harris, J. (2006) Environment

7. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 7 Johnson, et al. (2006) Element Ratios LMC Clusters MW Clusters Field, LMC MW dSph

8. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 8 An LMC Halo? Old stars found well beyond “standard” radius of LMC disk A. Saha, et al. Structure

9. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 9 A New Sense of Urgency... The clouds are not bound to the Milky Way (Kallivayalil, Alcock, et al.)?

10. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 10 SAGE and The Large Magellanic Cloud Add MLH to SFH+CEH -> Complete picture of a galaxy's evolution Life cycle of matter: Old stars ISM Y Stars Global SED, contributions from ext and point srcs Use the galaxy components to inform studies of SF at high redshift Bill Reach to cover ISM, extended emission Overview: Meixner et al. (2006); Evolved stars: Blum et al. (2006)

11. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 11 Spitzer Launch August 25, 2003 (day 1270) Mission life 5 yr+ (Cycle 4 last full cycle)

12. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 12 Spitzer 85 cm Telescope – DL 6.5um – LHe cooled (360 ltr) – Trailing Earth orbit (0.1 AU/yr) – Temp ~ 40 K

13. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 13 Spitzer Instruments IRAC (Infrared Array Camera), – 3.6 um, 4.5 um InSb – 6.5 um, 8.0 um SiAs – 5.12 arc minute FOV, 1.2'' pixels MIPS (Multi-band Imaging Photometer) – 128x128 SiAs 24 um, 32x32, 2x20 GeGa 70, 160 um – 2.5'', 5''/10'', 16'' pixels IRS (Infrared Spectrometer) – 5-40 um – R=50-600

14. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 14 Spitzer SAGE in context of other LMC surveys Two epochs: Jul/Aug 05, Oct/Nov 05, 500 hr MIPS bands: 24, 70, 160 um, Fast Scan map, 38 legs of 25'x4 deg 60, 30, 6 s per pixel. IRAC bands: 3.6, 4.5, 5.6, 8 um, 14x28 HDR 0.6s 12s; 43s per pixel in 1.1 deg tiles CO HIHI HIHI IRASH alpha/MIPS UVStars/IRAC UV IRAS 100 um Ha Stellar density MCELS, Smith, Points et al.

15. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 15 Previous IR surveys of LMC IRAS: 12, 25, 60, 100 um (Schwering 1989) – 8.5x8.5 degree coverage – 1 arc minute angular resolution – 1823 object point source list MSX: 8 um (Egan, van Dyk & Price 2001) – 10x10 degree coverage – 20'' angular resolution – 1806 object point source list 2MASS: J, H, Ks (Nikolaev & Weinberg 2000) & DENIS I, J, H, Ks (Cioni et al. 2000) – ~2'' angular resolution – 820,000; 1.3 million

16. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 16 IRAC Tile, 3.6, 4.5, 8.0

17. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 17 24 70 160 MIPS Scan Maps

18. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 18 IRAC 3.6, 4.5, 8.0 C

19. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 19 MIPS 24, 70, 160

20. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 20 Data for the community: SAGE as Legacy Original pipeline images released immediately Point source catalogs provided January, 2007. Available from SSC.

21. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 21 Hess Diagram LMC A-G SG Saturation J-band limit Foreground LMC OB TRGB AGB RGB

22. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 22 C-rich O-rich SG “Extreme” AGB, SG AGB->O-rich become C-stars during dredge up Lower Z, easier to get C/O > 1 Extreme stars mostly C-rich, but need spectra to decide

23. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 23 Models 1 Marigo (2002) C/O varies on TP-AGB Previous models used fixed, scaled solar opacity New models have variable opacities Net result, C stars move to lower Teff (O-rich stars don't)

24. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 24 Models 2 Ks J-Ks Cioni et al. (2006) use Marigo models to explain C-rich/O-rich loci in 2MASS CMD Define photometric selection of C-, M- stars

25. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 25 SAGE has IRAC plus 2MASS catalog, so we can define regions in NIR/MIR CMDs Four main evolved star types: – O-rich – C-rich – SG – Extreme O-rich C-rich SG Extreme [3.6] J - [3.6]

26. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 26 Spatial distributions match source types

27. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 27 J-K vs KJ-[3.6] vs [3.6] J-[8.0] vs [8.0] Probing Dusty Envelopes

28. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 28 Galaxies Lots of galaxies, “2MASS J-band drop outs”

29. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 29 SWIRE ELAIS N1 Approx 300 sources per square degree to [8.0]=13.5, Similar result using [8.0] and [24] Slightly more SAGE sources at [3.6], [8.0]

30. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 30 24 microns SG/L-AGB have larger excess than E stars See lower L mass losing sources -> cool, dusty envelopes IRS sources fall where expected Buchanan et al. (2006) O-rich C-rich

31. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 31 Lower Luminosity O-rich Mass Loss Sources Tip of AGB: [8.0] ~ 10.5 These stars have mdot (Msun/yr) ~ -7 to -6 Same core, increasing mdot (excess begins at [8.0])

32. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 32 Mass Loss Rates van Loon et al., (1999) ISO Spectra SAGE IRS

33. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 33 Mass Loss Rates Log10 (10 6 *Msun/yr) [24]

34. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 34 Sundar Srinivasan Derive Excess vs stellar core Match types to detailed mass loss rates Empirical Shell Properties

35. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 35 Carbon Rich AGB stars: 1.70E-03, 25% Oxygen Rich AGB stars: 1.70E-03, 25% Super giants ([3.6] < 10): 1.00E-03, 13% Extreme AGB: 2.60E-03, 37% Total: 7.00E-03, 100% Similar to SN rate (Chu & Kennicutt 1988) Mass Loss by type over Entire LMC (Msun/yr)

36. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 36 Kevin Volk Dust Shell Models

37. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 37 Model Grid Kevin Volk

38. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 38 Young Stellar Objects ?

39. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 39 Properties of Sources in a Large CO complex Entire CO clouds SFR Galactic UCHII Image courtesy of Rémy Indebetouw

40. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 40 Identifying and Analyzing on-going SF

41. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 41 12 CO from NANTEN, Fukui et al. Images courtesy of Rémy Indebetouw

42. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 42 N4 30” RGB=24,8,4.5um contours=cm continuum (RI et al. 2005) candidate YSOs: example 30'' Image courtesy of Rémy Indebetouw

43. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 43 Young Stellar Objects candidate YSOs: where? R: CO Fukui et al. G:HI Kim et al. (1998) B:4.8GHz Dickel et al. (2005) Image courtesy of Rémy Indebetouw

44. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 44 The Global SED * * * Evolved stars *

45. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 45 Summary SAGE closes the “observational loop” for galaxy evolution of the LMC, leveraging a vast archive of UV, Optical, IR, and radio data. SAGE detects ``all'' mass losing sources in galaxy Evolved stars are a very significant source of input to the ISM, new stars

46. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 46 Coming Soon: SAGE-SMC

47. February 15, 2007 R. Blum – NOAO-Steward Joint Colloquium 47